The very first caveat of our simulations is their 2.5-dimensional nature, as
our method naturally imposes axisymmetry to the Wolf-Rayet
nebulae [1]}, [2]}.
While this is acceptable in our pilot study, performing full 3D MHD models
better resolving the detailed formation of, e.g. instabilities during the
wind-wind interaction mechanisms [3]}, [4]}
should be considered in the future.
Secondly, we neglected several microphysical processes, such as
radiation transport in the close surroundings of the massive star.
The high temperatures of the Wolf-Rayet star (\(\sim 10^{5}\, \rm K\) ) must
affect the local thermodynamical properties and the energy budget of the
stellar wind, and, as radiation pressure is at work therein, this should
changes the gas dynamics [5]}.
Any chemical and/or non-ideal MHD mechanisms are also totally neglected
in our simulations. Their consideration, much beyond the scope of our simplistic
work, will be treated in follow-up studies.
Last, our study which continues the work of [3]},
utilises analytic prescriptions for the evolution of the stellar wind properties.
It has the advantage to directly use stellar properties derived
from e.g., observations of blue supergiant stars [7]}, [8]}, [9]}, [10]}, however, at the cost of the introduction
of free parameters such as the timescale \(\Delta t\)  of the corresponding
phase transition. This can be circumvented by using self-consistently calculated
theoretical stellar evolution models [11]}, [12]}.
